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Title:
Theoretical models of Cepheid variables and their BVI(c) colors and magnitudes
Authors:
Chiosi, C.; Wood, P. R.; Capitanio, N.
Affiliation:
AA(Padova Univ., Padua, Italy), AB(Mount Stromlo and Siding Spring Observatories, Canberra, Australia), AC(Padova Univ., Padua, Italy)
Publication:
Astrophysical Journal Supplement Series (ISSN 0067-0049), vol. 86, no. 2, p. 541-598. (ApJS Homepage)
Publication Date:
06/1993
Category:
Astrophysics
Origin:
STI
NASA/STI Keywords:
CEPHEID VARIABLES, STELLAR COLOR, STELLAR LUMINOSITY, STELLAR MAGNITUDE, STELLAR MASS, STELLAR OSCILLATIONS, BOLOMETERS, MAGELLANIC CLOUDS, STELLAR INTERIORS
DOI:
10.1086/191790
Bibliographic Code:
1993ApJS...86..541C

Abstract

Pulsation models for Cepheid variables have been constructed and used to derive PMR and associated relations and the positions of the instability strips. Theoretical quantities have been transformed into observational UBVR(c)I(c) magnitudes and colors. The instability strips for three modes of pulsation have been obtained, and analytical fits to the effective temperature and luminosity along the blue and red edges of the instability strips are presented. The use of new Cepheid models and of the mass-period-luminosity-color relations leads to a good determination of the pulsational mass of the Cepheid stars. The problem of mass discrepancy can likely be solved by the adoption of mild-to-large overshoot models to derive the evolutionary mass. It is suggested that abundance-dependent studies that rely on B-V as a color should be treated with caution. It is recommended that V-I be used as a color.

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